TA: David Lin Office hours: For help with Cepheid variable lab,

Slides:



Advertisements
Similar presentations
Weak Lensing of the CMB Antony Lewis Institute of Astronomy, Cambridge
Advertisements

© Gary Larson – The Far Side The Cosmic Microwave Background (CMB)
Challenges for the Standard Cosmology Tom Shanks Durham University.
Chapter 26: Cosmology Why is the sky dark? The expanding universe Beginning of the universe: The Big Bang Cosmic microwave background The early universe.
More on time, look back and otherwise t in R(t) starts from beginning of big bang Everywhere in universe starts “aging” simultaneously Observational.
If the universe were perfectly uniform, then how come the microwave background isn’t uniform? Where did all the structure(galaxies, clusters, etc.) come.
CMB: Sound Waves in the Early Universe Before recombination: Universe is ionized. Photons provide enormous pressure and restoring force. Photon-baryon.
Universe in a box: simulating formation of cosmic structures Andrey Kravtsov Department of Astronomy & Astrophysics Center for Cosmological Physics (CfCP)
The Cosmic Microwave Background. Maxima DASI WMAP.
Concluding Comments For the Course Cosmology Fascinating Past Highly accomplished present (for example, the material covered in this course). Really exciting.
Physics 133: Extragalactic Astronomy ad Cosmology Lecture 4; January
Prof. Mel Ulmer DEPT OF PHYSICS & ASTRONOMY
1 Announcements Cosmos Assignment 5, due Monday 4/26, Angel Quiz Monday, April 26 Quiz 3 & Review, chapters Wednesday, April 28, Midterm 3: chapters.
1 Announcements There will be a star map on the exam. I will not tell you in advance what month. Grades are not yet posted, sorry. They will be posted.
Cosmology Physics CSG Day at Southampton University 5/6/7 13.7Gyr ABB Steve King.
Prof. Mel Ulmer DEPT OF PHYSICS & ASTRONOMY Discussion sections begin meetings this week Begin.
Physics 133: Extragalactic Astronomy and Cosmology Lecture 14; March
Chapter 31 Galaxies & the Universe Review & Recap It does this by precisely measuring the speed of gas and stars around a black hole. This provides clues.
Dark Energy and Cosmic Sound Daniel Eisenstein (University of Arizona) Michael Blanton, David Hogg, Bob Nichol, Nikhil Padmanabhan, Will Percival, David.
Cosmic Microwave Background (CMB) Peter Holrick and Roman Werpachowski.
PHY306 1 Modern cosmology 4: The cosmic microwave background Expectations Experiments: from COBE to Planck  COBE  ground-based experiments  WMAP  Planck.
Early times CMB.
The Standard Model Part II. The Future of the Universe Three possible scenarios: Expand forever (greater than escape velocity) Expand to a halt (exactly.
AS2001 / 2101 Chemical Evolution of the Universe Keith Horne Room 315A
Our Evolving Universe1 Vital Statistics of the Universe Today… l l Observational evidence for the Big Bang l l Vital statistics of the Universe   Hubble’s.
University of Durham Institute for Computational Cosmology Carlos S. Frenk Institute for Computational Cosmology, Durham Galaxy clusters.
Dark Energy Wednesday, October 29 Midterm on Friday, October 31.
Hubble’s galaxy classes Spheroid Dominates Disk Dominates.
The measurement of q 0 If objects are observed at large distances of known brightness (standard candles), we can measure the amount of deceleration since.
Galaxy Dynamics Lab 11. The areas of the sky covered by various surveys.
The Expanding Universe. The Hubble Law The Hubble constant H o is one of the most important numbers in cosmology because it may be used to estimate the.
Latest Results from LSS & BAO Observations Will Percival University of Portsmouth StSci Spring Symposium: A Decade of Dark Energy, May 7 th 2008.
The Conspiracy That the dark matter conspire to just make the rotation curves nearly flat Bottom line: M/L 40 M O /L O from these “flat rotation curves”..
Cosmology and Dark Matter III: The Formation of Galaxies Jerry Sellwood.
Distances: mostly Unit 54
The Early Universe Thursday, January 24 (planetarium show tonight: 7 pm, 5 th floor Smith Lab)
More buzz words, etc. Structure evolution and types of WIMPS Bottom-up Cold Dark Matter (CDM) Top-Down Hot Dark Matter (HDM) “Cold” = “slow” = less then.
Universe Tenth Edition Chapter 25 Cosmology: The Origin and Evolution of the Universe Roger Freedman Robert Geller William Kaufmann III.
Lecture 27: The Shape of Space Astronomy Spring 2014.
The Fate of the Universe. The fate depends on the rate of expansion and the density Density greater than critical value – gravity will halt expansion.
Chapter 20 Cosmology. Hubble Ultra Deep Field Galaxies and Cosmology A galaxy’s age, its distance, and the age of the universe are all closely related.
Mini Review: Ocam’s Razor: Start out with simplest assumptions Hot Big Bang, Expanding Universe: Only baryonic matter => CMB existence, universe old and.
Astronomy 2 Overview of the Universe Spring Lectures on External Galaxies. Joe Miller.
The Growth of Structure
2dF Galaxy Redshift Survey ¼ M galaxies 2003
Simulated black hole picture
The Dark Universe Susan Cartwright.
Harrison B. Prosper Florida State University YSP
WEIGHING THE UNIVERSE Neta A. Bahcall Princeton University.
The Big Bang The Big Bang
17. 3 The Big Bang and Inflation 17
Harrison B. Prosper Florida State University YSP
ASTR Fall Semester [Slides from Lecture22]
Light: The Cosmic Messenger
4. Whole new worlds Continued from AstrophysicsDS#3
dark matter and the Fate of the Universe
More Fun with Microwaves
Cosmological Assumptions
Galaxies.
Images: M. Blanton. Images: M. Blanton Figures: M. Blanton & SDSS.
Dark Matter, Dark Energy, and the Fate of the Universe
Galaxies What is a galaxy?
Galaxies Chapter 16.
Homework #10 is due tonight, 9:00 pm.
The Big Bang The Big Bang
Measurements of Cosmological Parameters
CMB Anisotropy 이준호 류주영 박시헌.
Recombination t = 380 ky T = 4000 K
After Bellwork, Read the FYI on the “Cosmological Distance Ladder” then answer the two questions in your science journal.
6-band Survey: ugrizy 320–1050 nm
Presentation transcript:

TA: David Lin d-lin@northwestern.edu Office hours: For help with Cepheid variable lab, Make an appointment http://www.astro.edu/astro/faculty/ulmer/a01_fall2002.html Discussion section meetings start this week

Mpc = 3 million light years We are here Approximate direction of 400 km/sec relative to Virgo & Ursa Major Group Mpc = 3 million light years

=> After subtracting out 250 km/sec around the Galaxy (can ignore motion in local group), we get a motion with respect to the CMB close to this direction in the Local Super Cluster => it all fits with the CMB being “far away”

Where MAP goes “bad” First Peak Red model gives 20% to L

Update, notice L not needed by CMB yet

Get the MAP results first hand in this room, April 18, 2003, at 4:00 p Get the MAP results first hand in this room, April 18, 2003, at 4:00 p.m. or watch the new papers in early January 2003. Results could disagree with Supernovae! Also, Jan 18, same time same place come for same general topic

Concept of “Error Bars”: Any measurement must have an uncertainty assigned to it. e.g. my mass is [about] 70 kg plus or minus… 0.5 kg. =>If my mass were to be measured, 67% of the time the reading would be within 0.5 kg of 70 kg

<= wrong right =>

Position of first peak tells us the universe is flat!! But this depends on interpretation Why is flat or “not” flat such a key (and disturbing) issue? Remember “flat” => k = 0, W0 = 1; W0 = 1 means relatively (20 times) higher density compared to the density of ordinary matter (as predicted, we see even less)

Key to interpretation: Assume we can calculate angular size of CMB fluctuations

Matter and Size of Fluctuations: Key “buzz word” is Adiabatic = Light and Matter follow each other Assume some sound speed in the gas and some ordinary (baryonic) and non-baryonic matter are mixed together WITH LIGHT Mixed with light means Adiabatic in this context With this model, calculate the angular size and intensity of the CMB (redshifted light) fluctuations from “acoustic waves.”

Observer Angles appear larger for closed case versus open Photons free stream to the observer on geodesics analogous to lines of longitude to the pole. Thus the same angular scale represents a smaller physical scale in a closed universe. Wayne Hu

Angles appear even smaller for open case Acoustic features appear at harmonics of a fixed physical scale at last scattering, the sound horizon. Measurement of the angular scale that such features subtend on the sky can thus measure the curvature of the universe through an angular size distance test. Wayne Hu

Adiabatic Fluctuations, cont. Use theory to match observed galaxies and clusters CMB measurements Structure formation driven by “seeds” Can make it all work In part because the theory is so flexible

Keep adding things to make the model agree with observations Dark Energy non-baryonic matter (2 kinds) most of bayronic matter not seen (yet)

300 million light years on a side What we are looking for!! The “Goldilocks ordinary matter (not too hot and not too cold) so as not to have been detected yet 300 million light years on a side